Appendix I: Lunar and Planetary Missions
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Volcanic History of the Imbrium Basin: a Close-Up View from the Lunar Rover Yutu
Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu Jinhai Zhanga, Wei Yanga, Sen Hua, Yangting Lina,1, Guangyou Fangb, Chunlai Lic, Wenxi Pengd, Sanyuan Zhue, Zhiping Hef, Bin Zhoub, Hongyu Ling, Jianfeng Yangh, Enhai Liui, Yuchen Xua, Jianyu Wangf, Zhenxing Yaoa, Yongliao Zouc, Jun Yanc, and Ziyuan Ouyangj aKey Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China; bInstitute of Electronics, Chinese Academy of Sciences, Beijing 100190, China; cNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; dInstitute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China; eKey Laboratory of Mineralogy and Metallogeny, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou 510640, China; fKey Laboratory of Space Active Opto-Electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China; gThe Fifth Laboratory, Beijing Institute of Space Mechanics & Electricity, Beijing 100076, China; hXi’an Institute of Optics and Precision Mechanics, Chinese Academy of Sciences, Xi’an 710119, China; iInstitute of Optics and Electronics, Chinese Academy of Sciences, Chengdu 610209, China; and jInstitute of Geochemistry, Chinese Academy of Science, Guiyang 550002, China Edited by Mark H. Thiemens, University of California, San Diego, La Jolla, CA, and approved March 24, 2015 (received for review February 13, 2015) We report the surface exploration by the lunar rover Yutu that flows in Mare Imbrium was obtained only by remote sensing from landed on the young lava flow in the northeastern part of the orbit. On December 14, 2013, Chang’e-3 successfully landed on the Mare Imbrium, which is the largest basin on the nearside of the young and high-Ti lava flow in the northeastern Mare Imbrium, Moon and is filled with several basalt units estimated to date from about 10 km south from the old low-Ti basalt unit (Fig. -
Curiosity's Candidate Field Site in Gale Crater, Mars
Curiosity’s Candidate Field Site in Gale Crater, Mars K. S. Edgett – 27 September 2010 Simulated view from Curiosity rover in landing ellipse looking toward the field area in Gale; made using MRO CTX stereopair images; no vertical exaggeration. The mound is ~15 km away 4th MSL Landing Site Workshop, 27–29 September 2010 in this view. Note that one would see Gale’s SW wall in the distant background if this were Edgett, 1 actually taken by the Mastcams on Mars. Gale Presents Perhaps the Thickest and Most Diverse Exposed Stratigraphic Section on Mars • Gale’s Mound appears to present the thickest and most diverse exposed stratigraphic section on Mars that we can hope access in this decade. • Mound has ~5 km of stratified rock. (That’s 3 miles!) • There is no evidence that volcanism ever occurred in Gale. • Mound materials were deposited as sediment. • Diverse materials are present. • Diverse events are recorded. – Episodes of sedimentation and lithification and diagenesis. – Episodes of erosion, transport, and re-deposition of mound materials. 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 2 Gale is at ~5°S on the “north-south dichotomy boundary” in the Aeolis and Nepenthes Mensae Region base map made by MSSS for National Geographic (February 2001); from MOC wide angle images and MOLA topography 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 3 Proposed MSL Field Site In Gale Crater Landing ellipse - very low elevation (–4.5 km) - shown here as 25 x 20 km - alluvium from crater walls - drive to mound Anderson & Bell -
Copyrighted Material
Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
A Summary of the Unified Lunar Control Network 2005 and Lunar Topographic Model B. A. Archinal, M. R. Rosiek, R. L. Kirk, and B
A Summary of the Unified Lunar Control Network 2005 and Lunar Topographic Model B. A. Archinal, M. R. Rosiek, R. L. Kirk, and B. L. Redding U. S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001, USA, [email protected] Introduction: We have completed a new general unified lunar control network and lunar topographic model based on Clementine images. This photogrammetric network solution is the largest planetary control network ever completed. It includes the determination of the 3-D positions of 272,931 points on the lunar surface and the correction of the camera angles for 43,866 Clementine images, using 546,126 tie point measurements. The solution RMS is 20 µm (= 0.9 pixels) in the image plane, with the largest residual of 6.4 pixels. We are now documenting our solution [1] and plan to release the solution results soon [2]. Previous Networks: In recent years there have been two generally accepted lunar control networks. These are the Unified Lunar Control Network (ULCN) and the Clementine Lunar Control Network (CLCN), both derived by M. Davies and T. Colvin at RAND. The original ULCN was described in the last major publication about a lunar control network [3]. Images for this network are from the Apollo, Mariner 10, and Galileo missions, and Earth-based photographs. The CLCN was derived from Clementine images and measurements on Clementine 750-nm images. The purpose of this network was to determine the geometry for the Clementine Base Map [4]. The geometry of that mosaic was used to produce the Clementine UVVIS digital image model [5] and the Near-Infrared Global Multispectral Map of the Moon from Clementine [6]. -
Geologic Structure of Shallow Maria
NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir cular basins. -
L RES~ARCH Coljncll ·
NA~IOf\i'At ACADEMIES OF SCIENCE AND ENGiNEERING 7 ·.· ·.·. : NATIONAL RES~ARCH ColJNCll · of the UNITED STATES OF AMERICA UNITED• STATES NATIONAL COMMITTEEI . International Union of Radio Sden<:e Nationa.1 Radio Science Meeting 13-15 January 1982 · f l··.. ·· Sponsored by USNC/URSI in cooperation with r Institute of Electrical and Electronics Engineers University of· Colorado Boulder, Colorado U.S.A. ~· 1' National Radio Science Meeting 13-15 January 19 82 Condensed Technical Program TUESDAY, 12 JANUARY 0900 CCIR U.S. Study Group 5 OT 8-8 CCIR U.S. Study ,Gr.oup 6 Radio Building 2000-2400 USNC/URSI Meeting Broker Inn WEDNESDAY, 13 JANUARY 0900-1200 A-1 Time Domai~ 1-ieasurements CRl-42 B-1 Scattering CR2-28 B-2 Electromagnetic Theory CR2-28 C-1 Topics in Information Theory CR0-30 F-1 Propagation Theory and Models CR2-26 J-1 Millimeter-Wave Astronomy UMC Ballroom 1330-1700 A-2 Microwave/Millimeter Wave Measurements CRl-42 B-3 Antenna Theory and Practice CR2-28 B-4 Inverse Scattering CR2-6 C-2 Digital HF: Equaltz ation and Reiated CR0-30 Techniques E-1 EM Noise in the Sea CRl-40 F-2 Ground-Based Remote Sensing CR2-26 H-1 VLF-ELF Wave Injection Into the CRl-46 Magnetosphere J-2 Very Long Baseline Interferometry UMC 157 1700 Commission A Business Meeting CRl-42 Commission C Business Meeting CR0-30 Commission E Business Meeting CRl-40 Commission F Business Meeting CR2-26 Commission H Business Meeting CRl-46 1800-2000 Reception Engineering Center 2000-2200 IEEE Wave Propagation Standards Committee CRl-46 TH.URSDAY, 14 JANUARY 0830-1200 A-3 -
“Savage and Deformed”: Stigma As Drama in the Tempest Jeffrey R
“Savage and Deformed”: Stigma as Drama in The Tempest Jeffrey R. Wilson The dramatis personae of The Tempest casts Caliban as “asavageand deformed slave.”1 Since the mid-twentieth century, critics have scrutinized Caliban’s status as a “slave,” developing a riveting post-colonial reading of the play, but I want to address the pairing of “savage and deformed.”2 If not Shakespeare’s own mixture of moral and corporeal abominations, “savage and deformed” is the first editorial comment on Caliban, the “and” here Stigmatized as such, Caliban’s body never comes to us .”ס“ working as an uninterpreted. It is always already laden with meaning. But what, if we try to strip away meaning from fact, does Caliban actually look like? The ambiguous and therefore amorphous nature of Caliban’s deformity has been a perennial problem in both dramaturgical and critical studies of The Tempest at least since George Steevens’s edition of the play (1793), acutely since Alden and Virginia Vaughan’s Shakespeare’s Caliban: A Cultural His- tory (1993), and enduringly in recent readings by Paul Franssen, Julia Lup- ton, and Mark Burnett.3 Of all the “deformed” images that actors, artists, and critics have assigned to Caliban, four stand out as the most popular: the devil, the monster, the humanoid, and the racial other. First, thanks to Prospero’s yarn of a “demi-devil” (5.1.272) or a “born devil” (4.1.188) that was “got by the devil himself” (1.2.319), early critics like John Dryden and Joseph War- ton envisioned a demonic Caliban.4 In a second set of images, the reverbera- tions of “monster” in The Tempest have led writers and artists to envision Caliban as one of three prodigies: an earth creature, a fish-like thing, or an animal-headed man. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Annualreport2005 Web.Pdf
Vision Statement The Space Science Institute is a thriving center of talented, entrepreneurial scientists, educators, and other professionals who make outstanding contributions to humankind’s understanding and appreciation of planet Earth, the Solar System, the galaxy, and beyond. 2 | Space Science Institute | Annual Report 2005 From Our Director Excite. Explore. Discover. These words aptly describe what we do in the research realm as well as in education. In fact, they defi ne the essence of our mission. Our mission is facilitated by a unique blend of on- and off-site researchers coupled with an extensive portfolio of education and public outreach (EPO) projects. This past year has seen SSI grow from $4.1M to over $4.3M in grants, an increase of nearly 6%. We now have over fi fty full and part-time staff. SSI’s support comes mostly from NASA and the National Sci- ence Foundation. Our Board of Directors now numbers eight. Their guidance and vision—along with that of senior management—have created an environment that continues to draw world-class scientists to the Institute and allows us to develop educa- tion and outreach programs that benefi t millions of people worldwide. SSI has a robust scientifi c research program that includes robotic missions such as the Mars Exploration Rovers, fl ight missions such as Cassini and the Spitzer Space Telescope, Hubble Space Telescope (HST), and ground-based programs. Dr. Tom McCord joined the Institute in 2005 as a Senior Research Scientist. He directs the Bear Fight Center, a 3,000 square-foot research and meeting facility in Washington state. -
A Possible Albian Impact Crater at Murshid, Southern Oman
GeoArabia, Vol. 7, No. 4, 2002 Gulf PetroLink, Bahrain A possible Albian impact crater at Murshid, southern Oman Bruce Levell1, Pascal Richard2 and Folco Hoogendijk2, Petroleum Development Oman ABSTRACT During interpretation of a 3-D seismic survey in southern Oman a solitary, 2.5-km-wide circular basin with a central peak and raised rim was identified in the subsurface 35 km west of the Marmul oil field. The feature is the only one of its kind in the area. The basinal structure is probably of Late Cretaceous (Albian) age and the regional geology strongly suggests that it is neither a volcanic crater nor related to salt-dome tectonics or salt dissolution. It possibly represents a crater formed by a terrestrial impact event and has been named the Murshid crater. This report does not constitute a detailed investigation of the possible impact crater but rather records the 3-D seismic observations and the drilling that has taken place near the structure so far. INTRODUCTION During interpretation of a newly acquired 3-D seismic survey for oil exploration in southern Oman, a solitary 2.5-km-diameter circular basinal feature was identified as a possible impact structure and was named the Murshid crater. It lies 35 km west of the Marmul oil field in the South Oman Salt Basin (Figure 1). The center of the structure is at latitude 18º10’59"N, longitude 54º55’08”E, and it is buried at a depth of approximately 380 m below mean sea level (680 m below the ground surface). The authors are petroleum geologists who felt that the Murshid basinal structure needed reporting to the wider scientific community. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
8.5 X 13.5 Doublelines.P65
Cambridge University Press 978-0-521-74128-6 - Exploring the Solar System with Binoculars: A Beginner’s Guide to the Sun, Moon, and Planets Stephen James O’Meara’s Index More information Index Adams, John Couch, 96 Carrington, Richard C., 15 degree of condensation (DC) of, Agesinax, 24 Carroll, Lewis, 60 111–112 Aionwantha (Hiawatha), 45 Ceres, 70, 99–101 estimating the brightness of, Airy, George Biddell, 50, 51, 55 discovery and history as a planet, 111–112 Alcock, George, 116 99–100 In–Out method, 111 Allen, Richard Hinckley, 136 general description of, 99, Modified–Out method, 111–112 Alphonsus VI (King of Portugal), 104 100–101 experience helps in observing, 112 Andersen, Hans Christian, 92 how to find, 101 flaring in brightness, 111 Arago, Francois, 59 Chaikin, Andrew, 54 how to locate and identify, 110 Araki, Genichi, 116 Challis, James, 50 in history, relating to, 103–108 Arend, Silvio, 115 Chambers, George F., 8, 19 King David, 103 Aristotle, 65 Cheshire Cat, 60 Melville’s Moby-Dick, 107–108 Arlt, Rainer, 132 Children of God (cult), 108 Napoleon, 106 Arrehenius, Svente, 78, 79 Chinese Catalogue (Biot’s), 131–132 Shakespeare’s Julius Caesar, 103–104 Arter, T. R., 131 Cicero (Roman emperor), 77 the broadside of the comets of Asteroid Belt, 101 City of God, The, 90 1680 and 1682, 104 brightest objects in, 101–102 Collins, Peter, 116 the death of Julius Caesar, 104 asteroids Cometographia, 103 the Middle Ages, 104 2003 EH1, 131 comets, 103–117 the Old Testament?, 103 3200 Phaeton, 142 1P (Halley), 103, 109, 114–115, the whaling ship